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Ian U. Roederer (U. Michigan and JINA-CEE)
The environment of the r-process
Generous funding for my work has been provided by:
image: A. Mellinger (Central Michigan U.), M. Mateo (U. Michigan)
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Boylan-Kochin et al., Mon. Not. Roy. Astron. Soc., 462, L51 (2016)
How representative, cosmologically speaking, is the Local Group?
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Boylan-Kochin et al., Mon. Not. Roy. Astron. Soc., 462, L51 (2016)slices from the Illustris simulation
106 Mpc com
oving7 M
pc comoving
JWST = James Webb Space Telescope
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Boylan-Kochin et al., Mon. Not. Roy. Astron. Soc., 462, L51 (2016)slices from the Illustris simulation
106 Mpc com
oving7 M
pc comoving
The Local Group spans a larger volume than the HUDF at z < 3.
It is representative of matter density andnumber of halos with Mvir(z = 7) ≲ 2 x 109 M⦿
JWST = James Webb Space Telescope
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ultra-faint dwarf (UFD) galaxies
* have low luminosity (MV > −7 or so)* are dark-matter dominated* contain old, metal-poor stellar populations* contain metals
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Brown et al., Astrophys. J., 796, 91 (2014)
UFD UFDUFD
UFD UFDUFD
(GC) (GC) (GC)
(GC) (GC) (GC)
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Brown et al., Astrophys. J., 796, 91 (2014)
UFD UFDUFD
UFD UFDUFD
(GC) (GC) (GC)
(GC) (GC) (GC)
75% of the stars in these UFD galaxies had formed by z ~ 10.(Or, at least, very early.)
Elements all across the periodic table were already present.
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Reticulum II
MemberNon-memberUnconfirmedForeground
Basic properties of Ret II UFD galaxy
distance stellar mass
absolute mag. (MV) mass-to-light ratio
mean [Fe/H] [Fe/H] dispersion
30 kpc2600 M⦿
−2.7500 −2.60.5
Koposov et al., Astrophys. J. 805, 130 (2015)Bechtol et al., Astrophys. J. 807, 50 (2015)
Walker et al., Astrophys. J. 808, 108 (2015)
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Ji et al., Astrophys. J., 830, 93 (2016) [rescaled]IUR, unpublished
Ret IIhalo stars
[Fe/H]
[Eu/
Fe]
-4 -3 -2
-1
0
1
2
3
The heavy element enhancement in Ret II matches the r-II stars in the halo.
UFD stars
Highly r-process enhanced stars(“r-II stars”)
Ret II UFD
151.96Eu
europium63
see also Roederer et al., Astron. J, 151, 82 (2016)
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Roederer, Astron. J., 137, 232 (2009)
r-process enhanced stars
other stars
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Beniamini et al., Astrophys. J., 832, 149 (2016) [plus annotations]
mass of Eu produced per event (M⦿)
frequency of r-process events
per core-collapse SN
IGNORE
151.96Eu
europium63
n-ca
ptur
e
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Beniamini et al., Astrophys. J., 832, 149 (2016) [plus annotations]
mass of Eu produced per event (M⦿)
frequency of r-process events
per core-collapse SN
IGNORE+ One event per ~5000 CCSN.
Produces ~10-5 M⦿ of Eu.
This matches expectations fora merger of two neutron stars.
core-collapse SN:~10-8 M⦿ of Eu
+
151.96Eu
europium63
n-ca
ptur
e
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Fong et al., Astrophys. J., 769, 56 (2013) [plus annotations]
(star-forming)
(non star-forming)
What are the host galaxies of short gamma-ray bursts (GRBs)?
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NS/NS and NS/BH rate limitsderived from first
Advanced LIGO run
(predicted)
LIGO and Virgo Coll., ApJ. Let., 832, L21 (2016)Vangioni et al., MNRAS, 455, 17 (2016) [plus annotations]
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Côté et al., Astophys. J., 836, 230 (2017)
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photo: C. Hull (Carnegie Obs.) and J. Bailey (Leiden)
— versatile high/moderate/medium/low-resolution modes— wide-field (30’ diameter) — multi-object (up to 256 targets)
The Michigan/Magellan Fiber System (M2FS) is well-suited for this followup.
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Data collected in 6.7 hours with M2FS/MedRes (R~8,000)
Ret II
Proof of concept:M2FS/MedRes spectra
Roederer et al., in prep.137.327Babarium
56
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image: A. Mellinger (Central Michigan U.), M. Mateo (U. Michigan)
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* via TSIP ** for programs that support NASA missions and/or strategic goals*** research related to exoplanets has first priority
Multi-object optical spectrographs accessible to astronomers at U.S. institutions
Telescope(> 3m)
Multi-object spectrograph
HemisphereN S
Spectral resol.low med mod high
U.S. public access percentage (~2017)
LBT (2 x 8m) MODS 4%*
Keck II (10m) DEIMOS 17%**
SALT (9.2m) RSS 0%
Gemini-North (8m) GMOS 29%
Gemini-South (8m) GMOS 33%
MMT (6.5m) HectochelleHectospec 0%
Magellan II (6.5m) M2FS 0%
SOAR (4.2m) Goodman 30%
CTIO Blanco (4m) COSMOS 39%
AAT (3.9m) 2dF+HERMES2dF+AAOmega 3%*
WIYN (3.5m) Hydra 40%***
✓ ✓ ✓
✓ ✓ ✓ ✓✓✓✓ ✓ ✓✓
✓✓ ✓
✓✓ ✓ ✓
✓✓ ✓✓ ✓✓
✓✓ ✓✓✓ ✓ ✓✓✓ ✓✓✓ ✓
✓ ✓ ✓
Needed for this followup (especially in the LSST era): — large aperture (> 6 m) and — moderate spectral resolution (R > 8,000)
R ≲ 1,000R ≲ 8,000
R ≲ 20,000R ≳ 20,000
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LBT*(MODS)
Keck II**(DEIMOS)
Gemini-N(GMOS)Gemini-S
(GMOS)MMT
(Hectochelle,Hectospec)
Magellan II(M2FS)SOAR
(Goodman)
Blanco(COSMOS)
AAT*(HERMES,AAOmega)
WIYN***(Hydra)
Multi-object optical spectrographs accessible to astronomers at U.S. institutions
* via TSIP ** for programs that support NASA missions and/or strategic goals*** research related to exoplanets has first priority
U.S. community access
U.S. private access - about 30 institutions represented(total includes international partner shares)
(on telescopes with > 3m primary mirror)
SALT(RSS)
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Telescope(> 3m)
Multi-object spectrograph
HemisphereN S
Spectral resol.low med mod high
U.S. public access percentage (~2017)
LBT (2 x 8m) MODS 4%*
Keck II (10m) DEIMOS 17%**
SALT (9.2m) RSS 0%
Gemini-North (8m) GMOS 29%
Gemini-South (8m) GMOS 33%
MMT (6.5m) HectochelleHectospec 0%
Magellan II (6.5m) M2FS 0%
SOAR (4.2m) Goodman 30%
CTIO Blanco (4m) COSMOS 39%
AAT (3.9m) 2dF+HERMES2dF+AAOmega 3%*
WIYN (3.5m) Hydra 40%***
✓ ✓ ✓
✓ ✓ ✓ ✓✓✓✓ ✓ ✓✓
✓✓ ✓
✓✓ ✓ ✓
✓✓ ✓✓ ✓✓
✓✓ ✓✓✓ ✓ ✓✓✓ ✓✓✓ ✓
✓ ✓ ✓
* via TSIP ** for programs that support NASA missions and/or strategic goals*** research related to exoplanets has first priority
Multi-object optical spectrographs accessible to astronomers at U.S. institutions
R ≲ 1,000R ≲ 8,000
R ≲ 20,000R ≳ 20,000
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* via TSIP ** for programs that support NASA missions and/or strategic goals*** research related to exoplanets has first priority
Multi-object optical spectrographs accessible to astronomers at U.S. institutions
Telescope(> 3m)
Multi-object spectrograph
HemisphereN S
Spectral resol.low med mod high
U.S. public access percentage (~2017)
LBT (2 x 8m) MODS 4%*
Keck II (10m) DEIMOS 17%**
SALT (9.2m) RSS 0%
Gemini-North (8m) GMOS 29%
Gemini-South (8m) GMOS 33%
MMT (6.5m) HectochelleHectospec 0%
Magellan II (6.5m) M2FS 0%
SOAR (4.2m) Goodman 30%
CTIO Blanco (4m) COSMOS 39%
AAT (3.9m) 2dF+HERMES2dF+AAOmega 3%*
WIYN (3.5m) Hydra 40%***
✓ ✓ ✓
✓ ✓ ✓ ✓✓✓✓ ✓ ✓✓
✓✓ ✓
✓✓ ✓ ✓
✓✓ ✓✓ ✓✓
✓✓ ✓✓✓ ✓ ✓✓✓ ✓✓✓ ✓
✓ ✓ ✓
Needed for this followup (especially in the LSST era): — large aperture (> 6 m) and — moderate spectral resolution (R > 8,000)
R ≲ 1,000R ≲ 8,000
R ≲ 20,000R ≳ 20,000
There are no moderate or high resolution spectrographs on large-aperture telescopes accessible to astronomers at U.S. institutions.
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Ian U. Roederer
The environment of the r-process
and JINA-CEEUniversity of Michigan
Generous funding for my work has been provided by: